论文标题
辐射反馈和超新星的影响诱发了湍流对早期星系的影响
The Effects of Radiative Feedback and Supernova Induced Turbulence on Early Galaxies
论文作者
论文摘要
最近推出的詹姆斯·韦伯（James Webb）太空望远镜承诺在我们对第一批恒星和星系的理解中无与伦比的进步，但是意识到这种潜力需要宇宙学模拟，以捕获影响这些对象的关键物理过程。在这里，我们表明辐射转移和亚网格湍流混合就是两个这样的过程。 By comparing simulations with and without radiative transfer but with exactly the same physical parameters and subgrid turbulent mixing model, we show that tracking radiative transfer suppresses the Population III (Pop III) star formation density by a factor of approximately 4. In both simulations, $\gtrsim 90\%$ of Pop III stars are found in the unresolved pristine regions tracked by our subgrid model, which does a better job at modeling来自超新星的金属围绕原始核心核心的区域占据了数十名的MYRS以彻底混合。同时，辐射转移通过开发离子化气泡来抑制流行III星形成，从而减慢这些区域的气体积聚，并导致紧凑的高红色高速星系，这些星系被孤立的低质量卫星所包围。因此，湍流混合和辐射转移都是必须包括的必不可少的过程，以准确模拟原始星系的形态，组成和生长。
The recently launched James Webb Space Telescope promises unparalleled advances in our understanding of the first stars and galaxies, but realizing this potential requires cosmological simulations that capture the key physical processes that affected these objects. Here we show that radiative transfer and subgrid turbulent mixing are two such processes. By comparing simulations with and without radiative transfer but with exactly the same physical parameters and subgrid turbulent mixing model, we show that tracking radiative transfer suppresses the Population III (Pop III) star formation density by a factor of approximately 4. In both simulations, $\gtrsim 90\%$ of Pop III stars are found in the unresolved pristine regions tracked by our subgrid model, which does a better job at modeling the regions surrounding proto-galaxy cores where metals from supernovae take tens of Myrs to mix thoroughly. At the same time, radiative transfer suppresses Pop III star formation, via the development of ionized bubbles that slows gas accretion in these regions, and it results in compact high-redshift galaxies that are surrounded by isolated low mass satellites. Thus turbulent mixing and radiative transfer are both essential processes that must be included to accurately model the morphology, composition, and growth of primordial galaxies.
